A Quadruple Magnetic Source Model for Arcade Flares and X-Ray Arcade Formations outside Active Regions. II. Dark Filament Eruption and the Associated Arcade Flare

Details A Quadruple Magnetic Source Model for Arcade Flares and X-Ray Arcade Formations outside Active Regions. II. Dark Filament Eruption and the Associated Arcade Flare A Quadruple Magnetic Source Model for Arcade Flares and X-Ray Arcade Formations outside Active Regions. II. Dark Filament Eruption and the Associated Arcade Flare

Apr 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...551..586h&link_type=abstract

The Astrophysical Journal, Volume 551, Issue 1, pp. 586-596.

Astronomy and Astrophysics

Astronomy

23

Magnetohydrodynamics: Mhd, Sun: Filaments, Sun: Flares, Sun: Magnetic Fields, Sun: Prominences

Scientific paper

A 2.5-dimensional MHD simulation based on the quadruple magnetic source model (Uchida et al.) was performed to deal with a dark filament eruption and the associated arcade flare. The numerical results are summarized as follows:1. A partition-like dark filament containing longitudinal fields (in some cases, helical fields) is confined in the thin current sheet in a quadruple magnetic source field. The dark filament separates the oppositely directed magnetic loop systems squeezed from both sides and thus prevents the release of the stored magnetic energy via magnetic reconnection. Thinning of the current sheet finally leads to the tearing of the dark filament, and the onset of anomalous resistivity at the tearing point induces fast magnetic reconnection. 2. In the region above the reconnection point, the upward plasma acceleration occurs at the slow shock where stressed magnetic field lines are allowed to expand upward as the result of the magnetic reconnection. The dark filament with helical fields is accelerated upward in this expanding field structure with a rounded shape, which may correspond to coronal mass ejection (CME) containing the erupted dark filament. On the other hand, reconnected field lines below the reconnection point shrink to form magnetic arcade loops heated by adiabatic compression, which may correspond to the associated arcade flare.3. It is shown that the greater part of the stored magnetic energy goes into the kinetic energy of the upward coronal magnetic expansion, and the rest is used for the heating of the magnetic arcade. This may explain the fact that CME carries greater energy compared with the energy of the associated arcade flare.

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